Maximum mass of neutron stars and strange neutron-star cores

By J. Zdunik, P. Haensel. 2012

180 citations recorded by the source corpus.

Context. The recent measurement of mass of PSR J1614-2230 rules out most existing models of the equation of state (EOS) of dense matter with high-density softening due to hyperonization that were based on the recent hyperon-nucleon and hyperon-hyperon interactions, which leads to a “hyperon puzzle”. Aims. We study a specific solution of this hyperon puzzle that consists of replacing a too soft hyperon core by a sufficiently stiff quark core. In terms of the quark structure of the matter, one replaces a strangeness-carrying baryon phase of confined quark triplets, some of them involving s quarks, by a quark plasma of deconfined u, d, and s quarks. Methods. We constructed an analytic approximation that fits modern EOSs of the two flavor (2SC) and the color-flavor-locked (CFL) color-superconducting phases of quark matter very well. Then, we used it to generate a continuum of EOSs of quark matter. This allowed us to simulate continua of sequences of first-order phase transitions at prescribed pressures, from hadronic matter to the 2SC and then to the CFL state of color-superconducting quark matter. Results. We obtain constraints in the parameter space of the EOS of superconducting quark cores, EOS.Q, resulting from Mmax > 2 M� . These constraints depend on the assumed EOS of baryon phase, EOS.B. We also derive constraints that would

Subfields: Astronomy and Astrophysics, Geophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/07135089f062eab3f6cd7e9aa5fc16bad3341e48

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Citations in the corpus

What can be learned from a future supernova neutrino detection (2017, result): “That appears not to be the case with more recent EOS’s leading to exotic stars which can look, from the outside, very similar to neutron stars and have masses larger than ∼ 2 M [184, 185], compatible with the observations [186].”
Generic conditions for stable hybrid stars (2013, background): “[15], showing the effect of different nuclear matter EoSs and different transition densities.”
A new quark-hadron hybrid equation of state for astrophysics - I. High-mass twin compact stars (2014, methodology): “Our approach for the construction of a quark-hadron phase transition with large latent heat extends beyond the phenomenological model of Zdunik & Haensel (2013) and Alford et al. (2013), known as ZHAHP.”
A NICER View of PSR J0030+0451: Millisecond Pulsar Parameter Estimation (2019, background): “For other families of EOS, such as those involving quarks or hyperons in hybrid stars (e.g., Zdunik & Haensel 2013) or baryon resonances (Drago et al. 2014), the radius may be (highly) sensitive to increasing mass.”